Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission. (arXiv:1908.07551v1 [astro-ph.HE])

Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission. (arXiv:1908.07551v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_C/0/1/0/all/0/1">C. Simpson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abe_K/0/1/0/all/0/1">K. Abe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bronner_C/0/1/0/all/0/1">C. Bronner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayato_Y/0/1/0/all/0/1">Y. Hayato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ikeda_M/0/1/0/all/0/1">M. Ikeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ito_H/0/1/0/all/0/1">H. Ito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iyogi_K/0/1/0/all/0/1">K. Iyogi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kameda_J/0/1/0/all/0/1">J. Kameda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kataoka_Y/0/1/0/all/0/1">Y. Kataoka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kato_Y/0/1/0/all/0/1">Y. Kato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kishimoto_Y/0/1/0/all/0/1">Y. Kishimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marti_L/0/1/0/all/0/1">Ll. Marti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miura_M/0/1/0/all/0/1">M. Miura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moriyama_S/0/1/0/all/0/1">S. Moriyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mochizuki_T/0/1/0/all/0/1">T. Mochizuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakahata_M/0/1/0/all/0/1">M. Nakahata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakajima_Y/0/1/0/all/0/1">Y. Nakajima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakayama_S/0/1/0/all/0/1">S. Nakayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okada_T/0/1/0/all/0/1">T. Okada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okamoto_K/0/1/0/all/0/1">K. Okamoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orii_A/0/1/0/all/0/1">A. Orii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pronost_G/0/1/0/all/0/1">G. Pronost</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sekiya_H/0/1/0/all/0/1">H. Sekiya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shiozawa_M/0/1/0/all/0/1">M. Shiozawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sonoda_Y/0/1/0/all/0/1">Y. Sonoda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takeda_A/0/1/0/all/0/1">A. Takeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takenaka_A/0/1/0/all/0/1">A. Takenaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_H/0/1/0/all/0/1">H. Tanaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yano_T/0/1/0/all/0/1">T. Yano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akutsu_R/0/1/0/all/0/1">R. Akutsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kajita_T/0/1/0/all/0/1">T. Kajita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okumura_K/0/1/0/all/0/1">K. Okumura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">R. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xia_J/0/1/0/all/0/1">J. Xia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bravo_Berguno_D/0/1/0/all/0/1">D. Bravo-Berguño</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labarga_L/0/1/0/all/0/1">L. Labarga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_P/0/1/0/all/0/1">P. Fernandez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blaszczyk_F/0/1/0/all/0/1">F. d. M. Blaszczyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kachulis_C/0/1/0/all/0/1">C. Kachulis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kearns_E/0/1/0/all/0/1">E. Kearns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raaf_J/0/1/0/all/0/1">J. L. Raaf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">J. L. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wan_L/0/1/0/all/0/1">L. Wan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wester_T/0/1/0/all/0/1">T. Wester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sussman_S/0/1/0/all/0/1">S. Sussman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berkman_S/0/1/0/all/0/1">S. Berkman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bian_J/0/1/0/all/0/1">J. Bian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Griskevich_N/0/1/0/all/0/1">N. J. Griskevich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kropp_W/0/1/0/all/0/1">W. R. Kropp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Locke_S/0/1/0/all/0/1">S. Locke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mine_S/0/1/0/all/0/1">S. Mine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smy_M/0/1/0/all/0/1">M. B. Smy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobel_H/0/1/0/all/0/1">H. W. Sobel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takhistov_V/0/1/0/all/0/1">V. Takhistov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weatherly_P/0/1/0/all/0/1">P. Weatherly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ganezer_K/0/1/0/all/0/1">K. S. Ganezer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">J. Y. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lim_I/0/1/0/all/0/1">I. T. Lim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_R/0/1/0/all/0/1">R. G. Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodur_B/0/1/0/all/0/1">B. Bodur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scholberg_K/0/1/0/all/0/1">K. Scholberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walter_C/0/1/0/all/0/1">C. W. Walter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coffani_A/0/1/0/all/0/1">A. Coffani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drapier_O/0/1/0/all/0/1">O. Drapier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonin_M/0/1/0/all/0/1">M. Gonin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imber_J/0/1/0/all/0/1">J. Imber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mueller_T/0/1/0/all/0/1">Th. A. Mueller</a>, et al. (122 additional authors not shown)

Supernova detection is a major objective of the Super-Kamiokande (SK)
experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be
added to the detector, which will improve the ability of the detector to
identify neutrons. A core-collapse supernova will be preceded by an increasing
flux of neutrinos and anti-neutrinos, from thermal and weak nuclear processes
in the star, over a timescale of hours; some of which may be detected at SK-Gd.
This could provide an early warning of an imminent core-collapse supernova,
hours earlier than the detection of the neutrinos from core collapse. Electron
anti-neutrino detection will rely on inverse beta decay events below the usual
analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds
while maximising detection efficiency. Assuming normal neutrino mass ordering,
more than 200 events could be detected in the final 12 hours before core
collapse for a 15-25 solar mass star at around 200 pc, which is representative
of the nearest red supergiant to Earth, $mathrm{alpha}$Ori (Betelgeuse). At a
statistical false alarm rate of 1 per century, detection could be up to 10
hours before core collapse, and a pre-supernova star could be detected by SK-Gd
up to 600 pc away.

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